Superbubble dynamics in globular cluster infancy - II. Consequences for secondary star formation in the context of self-enrichment via fast-rotating massive stars

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Volume 552 (April 2013)

A&A, 552 (2013) A121

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Table 2

Properties of low-metallicity fast-rotating massive stars.

M_∗^a /	R_∗^b /	Ṁ_fast^c /	Ṁ_slow^d /	T_eq,start^e /	T_eq,end^f /	Δt_on^g /	Δt_off^h/	Q₀ⁱ /	Q_LW^j /
M _⊙	R _⊙	M_⊙ Myr^-1	M_⊙ Myr^-1	Myr	Myr	Myr	Myr	10³⁵erg s^-1	10⁴⁹s^-1

120	12	1	66	0.7	3.15	0.020	0.080	28	9
60	10	0.2	14	0.9	4.4	0.028	0.067	3.9	1.26
40	8	0.06	14	1.1	5.7	0.065	0.250	1.2	0.192

Notes.

^(a)

Mass of the star.

^(b)

Photospheric radius.

^(c)

Mass loss rate of the steady fast wind.

^(d)

Mass loss rate of the slow equatorial wind.

^(e)

Global time at which the intermittent equatorial ejections start.

^(f)

Global time at which the intermittent equatorial ejections end.

^(g)

Duration of the individual slow-wind episodes.

^(h)

Time span in between any two slow-wind episodes.

⁽ⁱ⁾

Total power of the steady, radiatively driven fast wind on the main sequence.

^(j)

Flux of Lyman-Werner photons (912 Å–1100 Å) at 1 Myr after reaching the main sequence; this is roughly constant during the main sequence.

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